The Infrared Imaging Spectrograph (IRIS) for TMT: instrument overview

The OpenSE Cookbook is an open-sourced collection of patterns, procedures, and best practices targeted for systems engineers who seek guidance on applying model-based and executable systems engineering (MBSE) using SysML. Its content has emerged from the system level modeling effort on the European Framework Program 6 (FP6) and the Thirty Meter Telescope (TMT). The TMT MBSE approach applied the Executable Systems Engineering Method (ESEM) and the open-source Engineering Environment (OpenMBEE) to specify, analyze, and verify requirements of TMT’s Alignment and Phasing System (APS) and the Narrow Field Infrared Adaptive Optics System (NFIRAOS). In these applications, implicit dependencies are made explicit in a formal model through the use of ESEM, OpenMBEE, and SysML modeling constructs. The value proposition for applying this MBSE approach was to establish precise requirements and fine-grained traceability to system designs, and to verify key requirements beginning early in development. The integration of ESEM and the OpenMBEE tooling infrastructure (providing linked-data and web-operability) is a significant added value for the MBSE approach. The APS is responsible for the overall pre-adaptive optics wavefront quality, using starlight to measure wavefront errors and align the TMT optics. In the formally integrated and executable SysML model, simulations are performed to analyze the impact of changed requirements and verify specified constraints for various operational scenarios. The APS team used several modeling patterns to capture information such as the requirements, the operational scenarios, involved subsystems and their interaction points, the estimated or required time durations, and the mass and power consumption. Adaptive optics systems are designed to sense real-time atmospheric turbulence and correct the telescope’s optical beam to remove its effect. The system model for the adaptive optics operational modes was developed to capture sequence behaviors and operational scenarios to run Monte-Carlo simulations for verifying acquisition time, observing efficiency, and operational behavior requirements. The model is particularly useful for investigating the effect of parallelization, identifying interface issues, and re-ordering sequence acquisition tasks. A former version of the Cookbook (which is now updated to MBSE challenges, goals, and lessons learned) included modeling guidelines and conventions for all system aspects, hierarchy levels, and views, which were developed during for the Active Phasing Experiment (APE), an opto-mechatronical system technology demonstrator for the Extremely Large Telescope (ELT). The Cookbook utilizes the above mentioned system models as real-world case-studies to demonstrate and document the applications of the recipes, providing also instructional examples and addressing the available tooling support. The Cookbook is accompanied by a number of SysML models and aodel libraries which facilitate model authoring and maintenance. The Cookbook covers the different aspects of Systems Engineering such as management of Requirements, Design (behavior and structure), Interfaces, Interdisciplinary Integration, Analysis, Trade Studies, and Technical Resources. This paper presents the background, motivation, architecture, and highlights some key content of the Cookbook. For example, interface management, error budget management, requirements verification, Monte Carlo driven analysis, and timing analysis of operational scenarios. The paper discusses how the capabilities of OpenMBEE contributed significantly to the adoption of executable systems engineering.

The scientific productivity of laser guide star adaptive optics systems strongly depends on the sky coverage, which describes the probability of finding natural guide stars for the tip/tilt wavefront sensor(s) to achieve a certain performance. Knowledge of the sky coverage is also important for astronomers planning their observations. In this paper, we present an efficient method to compute the sky coverage for the laser guide star multiconjugate adaptive optics system, the Narrow Field Infrared Adaptive Optics System (NFIRAOS), being designed for the Thirty Meter Telescope project. We show that NFIRAOS can achieve more than 70% sky coverage over most of the accessible sky with the requirement of 191 nm total rms wavefront.

The population of galaxies we see today is the result of billions of years of gas inflows, outflows, mergers, and feedback. To develop any holistic picture of the origin and evolution of galaxies, we thus need to understand their environments. The circumgalactic and intergalactic media (CGM and IGM) - the gas around and between galaxies, respectively - represent a large part of this environment. However, this gas is extremely faint and thus difficult to observe, and only recently have we been able to image it directly. This thesis presents instrumental and observational work focused on revealing galaxy environments in the early universe. Chapter 1 presents a brief history of our understanding of galaxies and an overview of our current picture of galaxy formation, including the role played by galaxy environments. In particular, it focuses on presenting the evolution of baryonic structures within a cosmological density field dominated by dark matter. Chapter 2 presents instrumental work on the Keck Cosmic Web Imager (KCWI, Morrissey et al. 2018), a new integral field spectrograph (IFS) for the Keck-2 10m telescope designed to study faint, extended emission. As an introduction, I discuss the advantages and disadvantages of integral field spectroscopy for the application of studying galaxy environments, as well as an overview of the prototype instrument - the Palomar Cosmic Web Imager (PCWI, Matuszewski et al. 2010). This chapter focuses primarily on engineering work during the development and testing of KCWI, though I conclude with a brief comparison of PCWI and KCWI performance in measuring the CGM around a high-redshift QSO. Chapter 3 presents the development of a software package designed to extract and analyze faint, extended emission in PCWI and KCWI data: CWITools. Although software is often an afterthought in astronomical and observational work, it is likely to become a primary barrier to conducting large IFS surveys of the CGM and IGM. This semi-automated analysis pipeline is presented and released publicly to empower future PCWI and KCWI studies. Chapter 4 presents the FLASHES (Fluorescent Lyman-α Structures in High-z Environments) pilot survey, published as O'Sullivan et al. 2020. The FLASHES pilot survey is an IFS study of extended HI Lyman-α emission in the environments of 48 z = 2.3 - 3.0 QSOs. The FLASHES Survey is the core project of this thesis, enabled by the instrumentation in Chapter 2 and the analysis pipeline developed in Chapter 3. The pilot survey represents the first statistically significant (N ≳ 30) sample of direct CGM observations in its redshift range. As such, it provides the first direct constraints on the 2D morphology, surface brightness profiles, and spatially resolved kinematics of the CGM during this period. Chapter 5 presents the first FLASHES follow-up study; deep IFS observations targeting extended Lyα 1216A, NV 1240A, CIV 1549A, and HeII 1640A emission from a subset of FLASHES pilot targets (O'Sullivan et al., in prep). Emission from metals in the CGM is expected to be an order of magnitude or more fainter than its Lyα, yet is a crucial ingredient in understanding the composition of the gas. Detecting this emission still requires multiple hours on 10m class telescopes. As such, large surveys of the multi-phase CGM remain extremely difficult to conduct. In this chapter, I present detections and upper limits of CGM metal emission around 8 FLASHES targets. Chapter 6 presents engineering work on FIREBall-2 (the Faint Intergalactic Redshifted Emission Balloon, second generation), a high-altitude UV telescope and IFS targeting CGM emission in the low-redshift universe (z ≃ 0.7). FIREBall-2 is an ambitious project deploying a novel, electron-multiplying CCD designed to achieve ≳ 50% quantum efficiency in the UV. This technology represents an order of magnitude increase in sensitivity from the microchannel plates used in the GALEX space telescope. FIREBall-2 serves as both an observational project in its own right, studying the low-z CGM, and a pathfinder mission for future UV space missions. Finally, Chapter 7 summarizes the contributions from this thesis and present a brief outlook on a few topics related to observations of galaxy environments.

FALCON: Extending adaptive corrections to cosmological fields

Blue Compact Dwarf (BCD) galaxies are metal-poor and gas-rich systems undergoing intense, spatially extended star-forming activity. These galaxies offer a unique opportunity to investigate dwarf galaxy formation and evolution, and probe violent star formation and its implications on the chemical, dynamical and structural properties of low-mass extragalactic systems near and far. Several fundamental questions in BCD research, such as their star formation histories and the mechanisms that control their cyclic starburst activity, are still far from well understood. In order to improve our understanding on BCD evolution, we are carrying out a comprehensive Integral Field Spectroscopic (IFS) survey of a large sample of BCDs. Integral Field Unit (IFU) spectroscopy provides simultaneously spectral and spatial information, allowing, in just one shot, to study the morphology and evolutionary status of the stellar component, and the physical properties of the warm interstellar medium (e.g., extinction, chemical abundances, kinematics). This ongoing IFS survey will supply much needed local templates that will ease the interpretation of IFS data for intermediate and high-redshift star-forming galaxies.

In this paper we describe the recent advances in the development of new technologies applied in the construction of Integral Field Units (IFUs) at Laboratorio Nacional de Astrofisica (LNA). Our prototype is the Eucalyptus lenslet IFU constructed for the 1.6m telescope at Pico dos Dias Observatory (OPD), Brazil. This first concept was the basis to build two other IFUs with significantly improved concepts: the SOAR Integral Field Unit Spectrograph (SIFS) and FRODOSPEC. All the new technologies used in the construction of these IFUs are described in detail in this paper and can be replicated in similar instruments with optical fibers, with considerable advantages over the traditional technologies.

<strong>11.1 Introduction</strong> Today, large-aperture modern telescope optical systems such as the ground-based Thirty Meter Telescope (TMT) and Giant Magellan Telescope (GMT) are divided into four parts: a large precision telescope radiation collector, a metrology and wavefront sensing and control (WFSC) system, the instrument that analyzes the complex wavefronts, and the detector that converts the complex wavefronts into intensity. Smaller-aperture space telescopes such as those used by the Wide-field Infrared Survey Explorer (WISE), Kepler, Stereo, and Ice, Cloud, and land Elevation Satellite (ICESat) do not require optical metrology and wavefront sensing and control because they are sufficiently small that their rigidity is obtained using mass, since the space system mass budget will accommodate it. In this chapter we expand the classical two-part astronomical optical system comprised of telescope and instrument into the much more capable (for large apertures) new three-part optical system of (1) the telescope, (2) the metrology and WFSC system, and (3) the instrument. At the heart of this new system is the two-stage optics system1 that collects, measures, and corrects the wavefront, and focuses it onto a field stop where the radiation passes into instruments that process the input complex wavefront for spectral, spatial (image), polarization, and radiometric information. In Chapters 8 and 9, we learned how scalar complex wavefronts propagate through an optical system to create an image, and we discussed the relationship between the wavefront and image quality. In Chapter 10, we learned that interferometry is a tool for analyzing the spectral (temporal) content and spatial structure of wavefronts. In this chapter, we show how wavefronts are manipulated to compensate for the following: <ul> &#x2022; telescope fabrication errors, &#x2022; the low mechanical stiffness characteristic of the new lightweight next-generation ground and space telescopes, and &#x2022; atmospheric turbulence. </ul>

An image slicer has been proposed for the Integral Field Spectrograph [1] of the 4-m European Solar Telescope (EST) [2] The image slicer for EST is called MuSICa (Multi-Slit Image slicer based on collimator-Camera) [3] and it is a telecentric system with diffraction limited optical quality offering the possibility to obtain high resolution Integral Field Solar Spectroscopy or Spectro-polarimetry by coupling a polarimeter after the generated slit (or slits). Considering the technical complexity of the proposed Integral Field Unit (IFU), a prototype has been designed for the GRIS spectrograph at GREGOR telescope at Teide Observatory (Tenerife), composed by the optical elements of the image slicer itself, a scanning system (to cover a larger field of view with sequential adjacent measurements) and an appropriate re-imaging system. All these subsystems are placed in a bench, specially designed to facilitate their alignment, integration and verification, and their easy installation in front of the spectrograph. This communication describes the opto-mechanical solution adopted to upgrade GRIS while ensuring repeatability between the observational modes, IFU and long-slit. Results from several tests which have been performed to validate the opto-mechanical prototypes are also presented.

Washburn Astronomical Laboratories of the University of Wisconsin-Madison Astronomy Department is developing a near infrared (NIR) integral field spectrograph for the 11-meter Southern African Large Telescope (SALT). This instrument will extend SALT’s capabilities into the NIR, providing medium resolution spectroscopy over the wavelength range of 0.8 to 1.7 microns. The integral field unit (IFU) is optimized for sampling nearby galaxies with an on-sky hexagonal extent of 24 x 28 arcsec containing 217 fibers of 1.33 arcsec diameter (median SALT seeing is 1.5 arcsec). Two separate blocks of 15 sky fibers are adjustable to distances ranging 54 to 165 arcsec from the IFU. This spectrograph, formerly known as RSS-NIR, was originally designed to mount at prime focus coupled to an optical spectrograph through a dichroic beam-splitter. The need to simplify telescope operations at prime focus prompted its reconfiguration into a fiber-fed, cooled, bench spectrograph, resulting in lower instrumental thermal background with a separate cooled collimator, stabilization of the pupil illumination in the spectrograph due to the azimuthal scrambling properties of fibers, and higher throughput at short wavelengths. Field-flattening and sky subtraction with the existing slit spectrograph has been challenging due to SALT’s varying pupil as the instrument payload tracks across the fixed primary mirror during observations. Simulations show that fiber scrambling of the pupil will improve the achievable sky subtraction residuals by 1-2 orders of magnitude. In this paper we present an overview of the reconfigured spectrograph design, its improved expected performance, and the new science drivers for NIR integral field spectroscopy.

We present the design and lab performance of a prototype lenslet-slicer hybrid integral field spectrograph (IFS), validating the concept for use in future instruments like SCALES/PSI-Red. By imaging extrasolar planets with IFS, it is possible to measure their chemical compositions, temperatures and masses. Many exoplanet-focused instruments use a lenslet IFS to make datacubes with spatial and spectral information used to extract spectral information of imaged exoplanets. Lenslet IFS architecture results in very short spectra and thus low spectral resolution. Slicer IFSs can obtain higher spectral resolution but at the cost of increased optical aberrations that propagate through the down-stream spectrograph and degrade the spatial information we can extract. We have designed a lenslet/slicer hybrid that combines the minimal aberrations of the lenslet IFS with the high spectral resolution of the slicer IFS. The slicer output f/\# matches the lenslet f/\# requiring only additional gratings.

We present the first results of an analysis of the properties of the molecular gas in the nuclear regions (r < 300 pc) of a sample of six nearby galaxies, based on new high spatial resolution observations obtained in the K-band with the near-infrared integral field spectrograph SINFONI at the Very Large Telescope. We derive two-dimensional distributions of the warm molecular and ionized gas from the H2, Br_gamma and HeI emission lines present in the spectra of the galaxies. We find a range of morphologies, including bar- and ring-like distributions and either centrally peaked or off-centre emission. The morphologies of the molecular and the ionized gas are not necessarily coincident. The observed emission-line ratios point towards thermal processes as the principal mechanism responsible for the H2 excitation in the nuclear and circumnuclear regions of the galaxies, independently of the presence of an active nucleus. We find that a rescaling of the H2 2.12 microns emission-line luminosity by a factor beta~1200 gives a good estimate (within a factor of 2) of the total (cold) molecular gas mass. The galaxies of the sample contain large quantities of molecular gas in their centres, with total masses in the ~ 105 - 108 Msol range. Never the less, these masses correspond to less than 3 per cent of the stellar masses derived for the galaxies in these regions, indicating that the presence of gas should not affect black hole mass estimates based on the dynamical modelling of the stars. The high-spatial resolution provided by the SINFONI data allowed us to resolve a circumnuclear ring (with a radius of ~270 pc) in the galaxy NGC 4536. The measured values of the Br_gamma equivalent width and the HeI/Br_gamma emission-line ratio suggests that bursts of star formation occurred throughout this ring as recently as 6.5 Myr ago.

Deployed as a multi-user shared facility on the 5.1 meter Hale Telescope at Palomar Observatory, the PALM-3000 highorder upgrade to the successful Palomar Adaptive Optics System will deliver extreme AO correction in the near-infrared, and diffraction-limited images down to visible wavelengths, using both natural and sodium laser guide stars. Wavefront control will be provided by two deformable mirrors, a 3368 active actuator woofer and 349 active actuator tweeter, controlled at up to 3 kHz using an innovative wavefront processor based on a cluster of 17 graphics processing units. A Shack-Hartmann wavefront sensor with selectable pupil sampling will provide high-order wavefront sensing, while an infrared tip/tilt sensor and visible truth wavefront sensor will provide low-order LGS control. Four back-end instruments are planned at first light: the PHARO near-infrared camera/spectrograph, the SWIFT visible light integral field spectrograph, Project 1640, a near-infrared coronagraphic integral field spectrograph, and 888Cam, a high-resolution visible light imager.

ABSTRACTWe describe the design, manufacture, commissioning, and performance of PMAS, the Potsdam Multi‐Aperture Spectrophotometer. PMAS is a dedicated integral field spectrophotometer optimized to cover the optical wavelength regime of 0.35–1 μm. It is based on the lens array–fiber bundle principle of operation. The instrument employs an all‐refractive fiber spectrograph, built with CaF2 optics, to provide good transmission and high image quality over the entire nominal wavelength range. A set of user‐selectable reflective gratings provides low to medium spectral resolution of approximately 1.5, 3.2, and 7 Å in first order, depending on the groove density (1200, 600, 300 grooves mm−1). While the standard integral field unit (IFU) uses a 16 × 16 element lens array, which provides seeing‐limited sampling in a relatively small field of view (FOV) in one of three magnifications (8″ × 8″, 12″ × 12″, or 16″ × 16″), a recently retrofitted bare fiber bundle IFU (PPak: PMAS fiber pack) expands the FOV to a hexagonal area with a footprint of 65″ × 74″. Other special features include a cryogenic CCD camera for field acquisition and guiding, a nod‐shuffle mode for beam switching and improved sky background subtraction, and a scanning Fabry‐Pérot etalon in combination with the standard IFU (PYTHEAS mode). PMAS was initially designed and built as an experimental traveling instrument with optical interfaces to various telescopes (Calar Alto 3.5 m, ESO VLT, LBT). It is offered as a common‐user instrument at Calar Alto under contract to MPIA Heidelberg since 2002.

The birefringent fiber optic image slicer design, or BiFOIS, adapts integral field spectroscopy methods to the special needs of high-sensitivity, spatially-resolved spectropolarimetry. In solar astronomy these methods are of particular importance, as dynamic magnetism lies at the heart of various multi-scaled phenomena in the solar atmosphere. While integral field units (IFU) based on fiber optics have been in continual development for some time, standard stock multimode fibers do not typically preserve polarization. The importance of a birefringent fiber optic IFU design stems from the need for dual-beam spatio-temporal polarimetric modulation to correct for spurious polarization signals induced either by platform jitter or atmospheric seeing. Here we characterize the polarization response of a second generation BiFOIS IFU designed for solar spectropolarimetry. The unit provides 60 × 64 spatial imaging pixels in a densely-packed, high filling factor configuration. Particular attention is placed on the spatial uniformity of the IFU polarization response. Calibrated first-light solar observations are also presented to demonstrate the performance of the device in a real application.

We investigate the dynamics of GN-z11, a luminous galaxy at z = 10.60, carefully analyzing the public deep integral field spectroscopy (IFS) data taken with the JWST NIRSpec integral field unit. While the observations of the IFS data originally targeted an He ii clump near GN-z11, we find that the C iii] λ λ1907, 1909 emission from ionized gas at GN-z11 is bright and spatially extended significantly beyond the point-spread function (PSF). The spatially extended C iii] emission of GN-z11 shows a velocity gradient with red- and blueshifted components in the north and south directions, respectively, which cannot be explained by the variation of the [C iii] λ1907/C iii] λ1909 line ratios. Assuming the velocity gradient is produced by disk rotation, we perform forward modeling with GalPak3D, including the effects of PSF smearing and line blending, and obtain a rotation velocity of vrot=257−117+138 km s−1, a velocity dispersion of σv=91−32+18 km s−1, and a ratio of vrot/σv=2.83−1.41+1.82 . The v rot/σv value would suggest a rotation-dominated disk existing at z > 10, albeit with large uncertainties. The rotation velocity agrees with those of numerical simulations predicting a rotating disk formed in the early Universe under the conditions of mass compaction and weak feedback. While the velocity gradient is consistent with the rotating-disk solution, we recognize that galactic outflows can also explain the velocity gradient, as well as the extended morphology and the high velocity dispersion found in the outskirts. Higher-signal-to-noise-ratio and higher-resolution data are necessary to conclude the physical origin of the velocity gradient in GN-z11.